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3 results on '"Caroline Soubiran"'

1. The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

Author

Shoko Jin, Scott C Trager, Gavin B Dalton, J Alfonso L Aguerri, J E Drew, Jesús Falcón-Barroso, Boris T Gänsicke, Vanessa Hill, Angela Iovino, Matthew M Pieri, Bianca M Poggianti, D J B Smith, Antonella Vallenari, Don Carlos Abrams, David S Aguado, Teresa Antoja, Alfonso Aragón-Salamanca, Yago Ascasibar, Carine Babusiaux, Marc Balcells, R Barrena, Giuseppina Battaglia, Vasily Belokurov, Thomas Bensby, Piercarlo Bonifacio, Angela Bragaglia, Esperanza Carrasco, Ricardo Carrera, Daniel J Cornwell, Lilian Domínguez-Palmero, Kenneth J Duncan, Benoit Famaey, Cecilia Fari na, Oscar A Gonzalez, Steve Guest, Nina A Hatch, Kelley M Hess, Matthew J Hoskin, Mike Irwin, Johan H Knapen, Sergey E Koposov, Ulrike Kuchner, Clotilde Laigle, Jim Lewis, Marcella Longhetti, Sara Lucatello, Jairo Méndez-Abreu, Amata Mercurio, Alireza Molaeinezhad, Maria Monguió, Sean Morrison, David N A Murphy, Luis Peralta de Arriba, Isabel Pérez, Ignasi Pérez-Ràfols, Sergio Picó, Roberto Raddi, Mercè Romero-Gómez, Frédéric Royer, Arnaud Siebert, George M Seabroke, Debopam Som, David Terrett, Guillaume Thomas, Roger Wesson, C Clare Worley, Emilio J Alfaro, Carlos Allende Prieto, Javier Alonso-Santiago, Nicholas J Amos, Richard P Ashley, Lola Balaguer-Nú nez, Eduardo Balbinot, Michele Bellazzini, Chris R Benn, Sara R Berlanas, Edouard J Bernard, Philip Best, Daniela Bettoni, Andrea Bianco, Georgia Bishop, Michael Blomqvist, Corrado Boeche, Micol Bolzonella, Silvia Bonoli, Albert Bosma, Nikolay Britavskiy, Gianni Busarello, Elisabetta Caffau, Tristan Cantat-Gaudin, Alfred Castro-Ginard, Guilherme Couto, Juan Carbajo-Hijarrubia, David Carter, Laia Casamiquela, Ana M Conrado, Pablo Corcho-Caballero, Luca Costantin, Alis Deason, Abel de Burgos, Sabrina De Grandi, Paola Di Matteo, Jesús Domínguez-Gómez, Ricardo Dorda, Alyssa Drake, Rajeshwari Dutta, Denis Erkal, Sofia Feltzing, Anna Ferré-Mateu, Diane Feuillet, Francesca Figueras, Matteo Fossati, Elena Franciosini, Antonio Frasca, Michele Fumagalli, Anna Gallazzi, Rubén García-Benito, Nicola Gentile Fusillo, Marwan Gebran, James Gilbert, T M Gledhill, Rosa M González Delgado, Robert Greimel, Mario Giuseppe Guarcello, Jose Guerra, Marco Gullieuszik, Christopher P Haines, Martin J Hardcastle, Amy Harris, Misha Haywood, Amina Helmi, Nauzet Hernandez, Artemio Herrero, Sarah Hughes, Vid Irsic, Pascale Jablonka, Matt J Jarvis, Carme Jordi, Rohit Kondapally, Georges Kordopatis, Jens-Kristian Krogager, Francesco La Barbera, Man I Lam, Søren S Larsen, Bertrand Lemasle, Ian J Lewis, Emilie Lhomé, Karin Lind, Marcello Lodi, Alessia Longobardi, Ilaria Lonoce, Laura Magrini, Jesús Maíz Apellániz, Olivier Marchal, Amparo Marco, Nicolas F Martin, Tadafumi Matsuno, Sophie Maurogordato, Paola Merluzzi, Jordi Miralda-Escudé, Emilio Molinari, Giacomo Monari, Lorenzo Morelli, Christopher J Mottram, Tim Naylor, Ignacio Negueruela, Jose Onorbe, Elena Pancino, Sébastien Peirani, Reynier F Peletier, Lucia Pozzetti, Monica Rainer, Pau Ramos, Shaun C Read, Elena Maria Rossi, Huub J A Röttgering, Jose Alberto Rubi no-Martín, Jose Sabater Montes, José San Juan, Nicoletta Sanna, Ellen Schallig, Ricardo P Schiavon, Mathias Schultheis, Paolo Serra, Timothy W Shimwell, Sergio Simón-Díaz, Russell J Smith, Rosanna Sordo, Daniele Sorini, Caroline Soubiran, Else Starkenburg, Iain A Steele, John Stott, Remko Stuik, Eline Tolstoy, Crescenzo Tortora, Maria Tsantaki, Mathieu Van der Swaelmen, Reinout J van Weeren, Daniela Vergani, Marc A W Verheijen, Kristiina Verro, Jorick S Vink, Miguel Vioque, C Jakob Walcher, Nicholas A Walton, Christopher Wegg, Anne-Marie Weijmans, Wendy L Williams, Andrew J Wilson, Nicholas J Wright, Theodora Xylakis-Dornbusch, Kris Youakim, Stefano Zibetti, Cristina Zurita, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, University of St Andrews. Centre for Contemporary Art, Universidad de Alicante. Departamento de Física Aplicada, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, and Astrofísica Estelar (AE)

Subjects
Astrofísica, Cosmology and Nongalactic Astrophysics (astro-ph.CO), NDAS, FOS: Physical sciences, Surveys, surveys, QB Astronomy, spectrographs [Instrumentation], observations [Cosmology], Instrumentation and Methods for Astrophysics (astro-ph.IM), Galaxy: general, stars: general, Solar and Stellar Astrophysics (astro-ph.SR), general [Galaxy], QC, QB, instrumentation: spectrographs, general [Stars], Análisis de datos, Instrumentation spectrographs, Astronomy and Astrophysics, general [Galaxies], galaxies: general, Astrophysics - Astrophysics of Galaxies, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), MCP, cosmology: observations, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366$-$959\,nm at $R\sim5000$, or two shorter ranges at $R\sim20\,000$. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for $\sim$3 million stars and detailed abundances for $\sim1.5$ million brighter field and open-cluster stars; (ii) survey $\sim0.4$ million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey $\sim400$ neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in $z1$ million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at $z>2$. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator., 41 pages, 27 figures, accepted for publication by MNRAS

Published
2023

2. Chemically Peculiar Stars in the Open Cluster Stock 2

Author

Marwan Gebran, Hervé Bouy, Marcel Agüeros, Laia Casamiquela, and Caroline Soubiran

Subjects
Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The recently re-discovered open cluster Stock 2, located roughly 375 pc away and about 400 Myr old, has the potential to be an exciting new testbed for our understanding of stellar evolution. We present results from a spectroscopic campaign to characterize stars near the cluster's main-sequence turnoff; our goal is to identify candidate chemically peculiar stars among the cluster's A stars. We obtained echelle spectra for 64 cluster members with ESPaDOnS on the 3.6-m Canada-France-Hawaii Telescope, Mauna Kea Observatory, USA, and for six stars with SOPHIE on the 1.93-m telescope at the Observatoire de Haute-Provence, France. We complemented these new observations with those of 13 high-mass cluster members from the HARPS-N archive; our overall sample is of 71 stars. We derived the fundamental parameters (Teff, log g, [M/H]) as well as vsini for our sample using the Sliced Inverse Regression (SIR) technique, and then used iSpec to derive individual abundances of 12 chemical species. With these abundance determinations, we identified nine A stars with anomalous levels of Sc, Ca, and other metallic lines. Follow-up observations of these Am candidates with a known age can transform them into benchmarks for evolutionary models that include atomic diffusion and help build a better understanding of the complex interactions between macroscopic and microscopic processes in stellar interiors., Accepted for publication in AJ

Published
2022

3. Structural parameters of 389 local Open Clusters

Author

Laia Casamiquela, Caroline Soubiran, Phillip Galli, Alfred Castro-Ginard, Yoann Tarricq, Javier Olivares, Nuria Miret Roig, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Soubiran, Caroline, Centre National D'Etudes Spatiales (France), Universidad de Barcelona, European Commission, Agencia Estatal de Investigación (España), and Ministerio de Ciencia, Innovación y Universidades (España)

Subjects
Astrophysics - instrumentation and methods for astrophysics, statistical [Methods], Astrophysics - astrophysics of galaxies, FOS: Physical sciences, Methods - statistical, Galaxy - structure, Surveys, 01 natural sciences, [SDU] Sciences of the Universe [physics], 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Galaxy: structure, Methods: statistical, Astrophysics::Galaxy Astrophysics, Open clusters and associations - general, general [Open clusters and associations], 010308 nuclear & particles physics, Galaxy - kinematics and dynamics, Astronomy and Astrophysics, Open clusters and associations: general, kinematics and dynamics [Galaxy], Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), Galaxy: kinematics and dynamics, structure [Galaxy]
Abstract

[Context] The distribution of member stars in the surroundings of an open cluster (OC) can shed light on the process of its formation, evolution, and dissolution. The analysis of structural parameters of OCs as a function of their age and position in the Galaxy constrains theoretical models of cluster evolution. The Gaia catalog is very appropriate for finding members of OCs at large distance from their centers. [Aims] We revisit the membership lists of OCs from the solar vicinity, in particular, by extending these membership lists to the peripheral areas through Gaia EDR3. We then take advantage of these new member lists to study the morphological properties and the mass segregation levels of the clusters. [Methods] We used the clustering algorithm HDBSCAN on Gaia parallaxes and proper motions to systematically search for members up to 50 pc from the cluster centers. We fit a King's function on the radial density profile of these clusters and a Gaussian mixture model (GMM) on their two-dimensional member distribution to study their shape. We also evaluated the degree of mass segregation of the clusters and the correlations of these parameters with the age and Galactic position of the clusters. [Results]. Our method performs well on 389 clusters out of the 467 clusters we selected, including several recently discovered clusters that were poorly studied until now. We report the detection of vast coronae around almost all the clusters and report the detection of 71 OCs with tidal tails. This multiplies the number of these structures that are identified by more than four. The size of the cores is smaller for old clusters than for young ones on average. Moreover, the overall size of the clusters seems to increase slightly with age, but the fraction of stars in the halo seems to decrease. As expected, the mass segregation is more pronounced in the oldest clusters, but no clear trend with age is evident. [Conclusions] OCs are more extended than previously expected, regardless of their age. The decrease in the proportion of stars populating the clusters halos highlights the different cluster evaporation processes and the short timescales they need to affect the clusters. Reported parameters such as cluster sizes or mass segregation levels all depend on cluster ages, but cannot be described as single functions of time., Y.T., C.S., and L.C. acknowledge support from “programme national de physique stellaire” (PNPS) and from the “programme national cosmologie et galaxies” (PNCG) of CNRS/INSU. L.C. acknowledges the support of the postdoc fellowship from French Centre National d’Etudes Spatiales (CNES). This work was (partially) supported by the Spanish Ministry of Science, Innovation and University (MICIU/FEDER, UE) through grant RTI2018-095076-B-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia ‘María de Maeztu’) through grant CEX2019-000918-M. J.O. acknowledges financial support from: (i) from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No 682903, P.I. H. Bouy), (ii) the French State in the framework of the “Investments for the future” Program, IdEx Bordeaux, reference ANR-10-IDEX-03-02, and iii) the Agencia Estatal de Investigación of the Ministerio de Ciencia, Innovación y Universidades through project PID2019-109522GB-C53.

Published
2021

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